Gamma Radiation From Flare-Accelerated Particles Impacting the Sun

Share, G. H.; Murphy, R. J.

doi:10.21236/ada594340

Cited by 5 publications

(3 citation statements)

References 21 publications

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“…As underlined , recently many interesting results were obtained in solar gamma-and X-ray spectroscopy and in investigations of ; (b) RHESSI data according to Share et al (2006): solid black curve with points -observed spectrum, dotted line -bremsstrahlung part, dashed curvecontribution of broad nuclear lines, dashed dotted curve -contribution of narrow nuclear lines (From Arkhangelskaja et al 2009) elemental abundances in the solar atmosphere. But only a few of them used data at energies higher than about 10 MeV.…”

Section: Conclusion and Discussion On Main Obtained Resultsmentioning

confidence: 94%

Solar Neutrons and Related Phenomena

Дорман¹

2010

Astrophysics and Space Science Library

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Section: Conclusion and Discussion On Main Obtained Resultsmentioning

confidence: 94%

Solar Neutrons and Related Phenomena

Дорман¹

2010

Astrophysics and Space Science Library

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“…The picture for flare ions remains less complete, partly because flares producing detectable γ-rays are much rarer but also because of the greater complexity of the nuclear radiation mechanisms. Ion acceleration in flares is studied via a variety of signatures at γ-ray wavelengths, consequences of nuclear reactions of primary accelerated ions with ambient nuclei (Share and Murphy, 2006;Murphy et al, 2007;Vilmer, MacKinnon, and Hurford, 2011): nuclear de-excitation lines in the 0.4 − 7 MeV range, excited by ions of 1 − 100 MeV/nucleon (Ramaty, Kozlovsky, and Lingenfelter, 1979;Kozlovsky, Murphy, and Ramaty, 2002); 2.223 MeV neutron capture and 511 keV positron annihilation lines, each resulting from ions spanning a wide energy range, from a few to 100s of MeV/nucleon (Lockwood, Debrunner, and Ryan, 1997;Hua et al, 2002;Kozlovsky, Lingenfelter, and Ramaty, 1987;Kozlovsky, Murphy, and Ramaty, 2002;Murphy et al, 2007); continuum radiation in the 0.1 MeV range, resulting from pion decay products of 0.2 − 0.3 GeV/nucleon ions (Dermer, 1986b;Murphy, Dermer, and Ramaty, 1987;Mandzhavidze and Ramaty, 1992;Vilmer et al, 2003). Energetic neutrons detected in space or with ground-based instruments also give information on accelerated flare ions (Chupp et al, 1987;Kocharov et al, 1998;Watanabe et al, 2006, e.g.…”

Section: Introductionmentioning

confidence: 99%

Self-consistent Modeling of Gamma-ray Spectra from Solar Flares with the Monte Carlo Simulation Package FLUKA

et al. 2019

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We use the Monte Carlo particle physics code FLUKA (Fluktuierende Kaskade) to calculate γ-ray spectra expected from solar flare energetic ion distributions. The FLUKA code includes robust physics-based models for electromagnetic, hadronic and nuclear interactions, sufficiently detailed for it to be a useful tool for calculating nuclear de-excitation, positron annihilation and neutron capture line fluxes and shapes, as well as ≈ GeV continuum radiation from pion decay products. We show nuclear de-excitation γ-ray line model spectra from a range of assumed primary accelerated ion distributions and find them to be in good agreement with those found using the code of Murphy et al. (2009). We also show full γ-ray model spectra which exhibit all the typical structures of γ-ray spectra S.

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“…In particular, this quasicontinuum component has a strong impact on the determination of the accelerated heavy-ion component which, due to the large Doppler broadening of the emitted γ -ray lines, produces similar quasicontinuum spectral features. Attempts have been made to extract the heavy-ion component from SF γ -ray spectra observed by SMM [49] interacting with interstellar matter in the inner Galaxy. The energies of γ -ray lines analyzed in this work are indicated by vertical labels in units of keV.…”

Section: Calculation Of the Total Nuclear γ-Ray Fluxes In Interactions Of Lecrs In The Inner Galaxymentioning

confidence: 99%

Measurement and analysis of nuclear γ -ray production cross sections in proton interactions with Mg, Si, and Fe nuclei abundant in astrophysical sites over the incident energy range E=30–66 MeV

Yahia-Chérif¹,

Ouichaoui²,

Kiener³

et al. 2020

Phys. Rev. C

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The modeling of nuclear γ -ray line emission induced by highly accelerated particles in astrophysical sites (e.g., solar flares, the gas and dust in the inner galaxy) and the comparison with observed emissions from these sites needs a comprehensive database of related production cross sections. The most important reactions of protons and α particles are those with abundant target elements like C, O, N, Ne, Mg, Si, and Fe at projectile energies extending from the reaction threshold to a few hundred MeV per nucleon. In this work, we have measured γ -ray production cross section excitation functions for 30, 42, 54, and 66 MeV proton beams accelerated onto nat C, C + O (Mylar), nat Mg, nat Si, and 56 Fe targets of astrophysical interest at the Separated Sector Cyclotron (SSC) of iThemba LABS (near Cape Town, South Africa). The AFRODITE array equipped with eight Compton suppressed high-purity (HPGe) clover detectors was used to record γ -ray line energy spectra. For known, intense lines previously reported experimental data measured up to E p 25 MeV at the Washington and Orsay tandem accelerators were thus extended to higher proton energies. Our experimental data for the last three targets are reported here and discussed with respect to previous data and to the Murphy et al. compilation [Astrophys. J. Suppl. Ser. 183, 142 (2009)], as well as to the predictions of the nuclear reaction code TALYS. The overall agreement between theory and experiment obtained in first-approach calculations using default input parameters of TALYS has been appreciably improved by using modified optical model potential (OMP), level deformation, and level density parameters. The OMP parameters have been extracted from theoretical fits to available experimental elastic and inelastic nucleon scattering angular distribution data by means of the coupled-channels reaction code OPTMAN. Experimental data for several new γ -ray lines are also reported and discussed. The astrophysical implications of our results are emphasised.

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Gamma Radiation From Flare-Accelerated Particles Impacting the Sun

Cited by 5 publications

References 21 publications

Solar Neutrons and Related Phenomena

Solar Neutrons and Related Phenomena

Self-consistent Modeling of Gamma-ray Spectra from Solar Flares with the Monte Carlo Simulation Package FLUKA

Measurement and analysis of nuclear γ -ray production cross sections in proton interactions with Mg, Si, and Fe nuclei abundant in astrophysical sites over the incident energy range E=30–66 MeV

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